标题： QUBIC I：概述和科学计划 显示英文标题

标题： QUBIC I: Overview and ScienceProgram

摘要： QUBIC是一种新型的偏振计，专门优化用于测量宇宙微波背景的B模式偏振，这是观测宇宙学的主要挑战之一。信号预计在几纳开尔文的数量级，容易受到仪器系统效应的影响，并被各种天体物理前景污染，这些只能通过多色观测来控制。QUBIC设计的独特能力在于结合了干涉测量在控制仪器系统效应方面的优势，以及热辐射计探测器在宽频带、背景限制灵敏度方面的优势。QUBIC合成光束具有频率依赖的形状，允许在仪器的两个物理波段（150 GHz和220 GHz）内多个子波段生成CMB偏振图。这种独特的能力使QUBIC与其他仪器区分开来，并使其特别适合表征和去除银河系前景污染。在本文中，作为八篇系列文章的第一篇，我们概述了QUBIC仪器设计、校准活动的主要结果，并介绍了QUBIC的科学计划，包括原初B模式和银河系前景的测量。我们给出了典型观测和测量的预测：假设三年的积分时间，假设从我们在阿根廷的站点完美去除前景并保持稳定的大气条件，我们的模拟显示，我们可以实现对有效张量-标量比（包括原初和前景B模式）的统计灵敏度$\sigma(r)=0.015$。假设220 GHz用于减去前景污染，并结合其他调查的数据，如Planck 353 GHz通道的数据，我们对原初张量的灵敏度由150 GHz通道单独给出，为$\sigma(r)=0.021$。 显示英文摘要

摘要： QUBIC is a novel kind of polarimeter optimized for the measurement of the B-mode polarization of the Cosmic Microwave Background, one of the major challenges of observational cosmology. The signal is expected to be of the order of a few tens of nK, prone to instrumental systematic effects and polluted by various astrophysical foregrounds which can only be controlled through multichroic observations. QUBIC is designed to address these observational issues with its unique capability to combine the advantages of interferometry in terms of control of instrumental systematic effects with those of bolometric detectors in terms of wide-band, background-limited sensitivity. The QUBIC synthesized beam has a frequency-dependent shape that allows producing maps of the CMB polarization in multiple sub-bands within the two physical bands of the instrument (150 and 220 GHz). This unique capability distinguishes QUBIC from other instruments and makes it particularly well suited to characterize and remove Galactic foreground contamination. In this article, first of a series of eight, we give an overview of the QUBIC instrument design, the main results of the calibration campaign, and present the scientific program of QUBIC including the measurement of primordial B-modes and Galactic foregrounds. We give forecasts for typical observations and measurements: with three years of integration, assuming perfect foreground removal and stable atmospheric conditions from our site in Argentina, our simulations show that we can achieve a statistical sensitivity to the effective tensor-to-scalar ratio (including primordial and foreground B-modes) $\sigma(r)=0.015$. Assuming the 220 GHz is used to subtract foreground contamination together with data from other surveys such as Planck 353 GHz channel, our sensitivity to primordial tensors is given by that of the 150 GHz channel alone and is $\sigma(r)=0.021$.